Speaker
Description
The population of massive, dust-obscured galaxies plays an increasingly prominent role in the context of galaxy evolution. These galaxies are considered the progenitors of the passive systems observed at z~3, and they significantly contribute to the cosmic star formation rate (SFR) density at high redshift (z>3). Due to their faintness in optical and near-infrared (NIR) bands, a key challenge is the selection of statistically significant samples of these objects.
Recent studies have shown that an effective approach for identifying these galaxies involves targeting radio-detected sources lacking counterparts in optical/NIR observations. While previous results have mainly been obtained from high-frequency radio data (e.g., 3 GHz), we extend this approach to lower frequencies by leveraging recent deep LOFAR 150 MHz observations in the Euclid Deep Field North (EDFN). Exploiting the Euclid Q1 data release, we identified a sample of 81 sources without detected counterparts up to Euclid/NISP H band.
Combining data from Euclid/VIS and NISP with multiwavelength observations from the Spitzer/IRAC, WISE, Herschel and LOFAR 150 MHz, we aim to derive the physical properties through spectral energy distribution fitting. This includes estimates of their SFRs, stellar masses, and photometric redshifts. Finally, we plan to infer their contribution to the SFR density and compare our results with those from NIR-dark samples selected using higher-frequency radio data. This comparison will allow us to investigate potential differences in redshift distribution and assess their position relative to the Main Sequence of star-forming galaxies.
